Post on 24-Dec-2021
Imaging with Micado at the E-ELT
Renato Falomo
INAF – Observatory of Padova, Italy
WORKSHOP: Imaging at the E-ELT
29 May 2009, Garching
FP7-N4 – Wide field imaging at the E-ELT – Garching 2009 May 29
Resolved stellar population in Virgo (high SB)
Detailed View of high redshift galaxies
MICADO – Main characteristics
Wavelength range : (0.6)-0.8 to 2.5 mic I, Y, J, H, Ks
Field of View : 53 x 53 arcsec
Pixel scale : 3 mas
PSF : FWHM 6(J) , 10(Ks) mas
: Strehl 0.015(I) 0.13(J) 0.47(Ks) : Strehl 0.015(I) 0.13(J) 0.47(Ks)
: EE(10mas) 0.10(J) 0.22(Ks)
Overall Throughput
40 %
Telescope + instrument + detector
MICADO – Expected performance
AB mag limits for isolated point sources
J(AB) = 30 in 5h (S/N=5) K(AB) = 29.5 in 5h (S/N=5)
Resolved Stellar Populations in Distant Galaxies
SFH from analysis of stellar distribution
on the CMD using stellar evolution theory
Best diagnostic from MS TOs where
different luminosities sample different
stellar ages, but old TOs are very faint
Old SPs can be sampled on the bright
RGB, at ~ 7 mags brighter, a gain
in volume of a factor of ~ 15 106
SCIENCE CASE FOCUSSES ON
DERIVING SFH FROM THE INTRINS.
BRIGHTEST PORTION OF THE CMD
Probe as much as possible distant SP
The Goal of Resolved Stellar Populations
The closest rich cluster of galaxiesVIRGO cluster ( DM = 31 )
THE METHOD
Simulation of a Stellar Population with ages between 0 and 12 Gyrand metallicity between 0.02 and 1 times solar (IMF by Kroupa)Code ZVAR (Bertelli et al. 92 + updates) Selected Areas in the CMD in order to:
• Sample specific AGE ranges
• Minimize effects of photometric errors
• Include enough objects for statistics3x10
7 M☼ 1.3x10
9 M☼
In each area:
from Stellar EvolutionGreggio 2002, ASPC 274 444
Counting stars in selected boxes
GIVES STELLAR MASS IN THE
SPECIFIC AGE RANGE
MICADO – The science caseAETC
Simulation and testing: possible observation
MICADO
FoV
M99 spiral galaxy in Virgo cluster
MICADO – The scienceResolved stellar population in distant galaxies
Simulation and testing
Stellar population : constant SFR ( Age 0 to 12 Gyr)
FoV = 3x3 arcsec ( 0.003 x FoV )
Distance module = 31 (Virgo cluster )
All stars with M(J) < -3.5 (Vega mag)All stars with M(J) < -3.5 (Vega mag)
Case A
70000 stars
Average SB : µ(K) ∼ 18
J(AB) <28.5
MICADO – Expected performance
Instrument parameters
Collecting area m2 1360
Telescope throughput 0.7
AO throughput 0.80
Instrument throughput 0.60
Total throughput 0.35
read out noise e- 5
instrumental background e-/s 0.1
pixel size mas 3
MICADO @E-ELT - SimulationAETC
Simulation and testing: NEW Maory PSF
• Six LGS• Seeing 0.6 arcsec• J 2.98 mas• J 2.98 mas• K 5.3 mas•SR = 0.6 (K) • Central 3 arcsec (constant PSF)
MICADO @E-ELT - SimulationResolved stellar population in distant galaxies
Simulation and testing: Maory PSF
70000 stars
MICADO : K filter – 5 h
FoV = 3x3
arcsec
MICADO : J filter – 5 h
MICADO – The scienceResolved stellar population in Virgo galaxies
Simulation and testing: Maory PSF
Central FoV
0.9x0.6
MICADO : K filter – 5 h
0.9x0.6 arcsec
MICADO : J filter – 5 h
MICADO@E-ELT - Simulation
Simulation and testing : Photometric analysis
Photometry performed by L. Bedin @ STScI without any knowledge of the simulated data
Comparison of simulated vs observed data
RESULTS:
• Catalogue of detected objects
• X, Y positions
• magnitude in J and K bands
• photometric additional parameters
• analysis NOT yet optimized
MICADO@E-ELT - Simulation
Simulation and testing : Photometric analysis by L. Bedin @ STScI
Comparison of
simulated vs
observed
magnitudemagnitude
K band
MICADO@E-ELT - Simulation
Simulation and testing : Photometric analysis
Photometric
accuracy
< 0.1 mag< 0.1 mag
for J<28.5
MICADO@E-ELT - Simulation
Simulation and testing : Photometric analysis
Completeness
Completeness
> 90% up to
J(AB) ∼ 28.5
> 70% up to
J(AB) ∼ 29.5
MICADO@E-ELT - Simulation
Simulation and testing : Photometric analysis
Calibrated
observed
CMD from
macthed macthed
stars
J(AB) <28.5
MICADO@E-ELT - Simulation
Simulation and testing : Photometric analysis
MICADO@E-ELT - Simulation
Simulation and testing : Photometric analysis
MICADO@E-ELT - Simulation
Simulation and testing : Photometric analysis
Simulated Observed Difference%
RSG 13 13 0
BSG 49 61 +25 %
Recovering the stellar mass in selected boxes
AGB 26 26 0
RGB 1901 1828 -4 %
Full numbers are x 300since this is a small fraction of Micado FOV
Near-IR images by MICADO @ E-ELT are able to determine the STELLAR MASS of different populations in galaxies of the Virgo cluster
NIR Imaging Camera in the next decade
MICADO @ E-ELT (42m)
WIRC @ TMT (30m)
NIRCam @ JWST (6m)
Imaging @ GMT
E-ELT (OWL)
JWST
NIRCam - JWSTMain properties
Main mirror (JWST): 6.5m
Resolution : 90 mas (K)
Platescale : 0.0317 "/pixel
FoV : 2.3‘ x 4.6’'
Wavelength range: 0.6 – 5 micronWavelength range: 0.6 – 5 micron
Background : ∼ Zodiacal light PSF
Micado@ELT vs NIRCam@JWST
K filter
(2.1 micron)
MICADO
E-ELT
NIRCam
JWSTBackground
(ABmag)15-15.5 ∼23
PS Sensitivity 29.5 - 30 30 – 30.5PS Sensitivity
(5h; S/N=5)
ABmag
29.5 - 30 30 – 30.5
Spatial Resolution
(FWHM)
mas
∼10 90
Field of View
arcmin2∼0.3 ~10
The study of stellar populations: Crowding limits
MICADO@E-ELT vs NIRCam@JWST
(K filter, FoV 3x3 arcsec )
MICADO E-ELT NIRCam JWST
The study of stellar populations: Crowding limits
MICADO@E-ELT vs NIRCam@JWST
(K filter, FoV 0.9x0.6 arcsec )
MICADO E-ELTNIRCam JWST
Resolved stellar populations in Virgo galaxies
Micado@E-ELT
offers a unique capability to investigate the
stellar population in the in crowded fields of stellar population in the in crowded fields of
distant galaxies (up to Virgo cluster)
MICADO view of high z galaxies
MICADO view of high z galaxies
MICADO view of high z galaxies
M(V) = -21
Re = 5 kpc
Redshift : 1-5
Example 1
Galaxy template -� simulated images
SB dimming (1+z)4
Size evolution helps a lot
to detect high z galaxies
Include k-correction & filter
tranfsormation
MICADO view of high z galaxies
Z=4
Z=5 Mv = -21
Re = 5 kpc
H band
5 hours
SIMULATION
0.1 0.3 0.5 arcsec
Z=1
Z=2
Z=35 hours
MICADO view of high z galaxies
Size 0.3 “
SIMULATION
Z = 2
Z = 1
MICADO view of high z galaxies
Size 0.3 “
SIMULATION
Z = 4
Z = 3
MICADO view of high z galaxies
SIMULATION
Z = 4 size = 0.3“Z = 4 size = 0.1“
Spiral galaxy at z = 2 Re 5kpc (0.3”)H band -- 5h SIMULATION
MICADO@ELT NIRcam@JWST
ELT view of high redshift galaxies
MICADO @ E-ELT will be able to characterize the
properties (incl. morphology ) of high redshift
galaxies and study their environments.
Near-IR (rest-optical) observations yield direct
comparison with the local Universe (in the optical)comparison with the local Universe (in the optical)
The E-ELT high ( 10mas ) angular resolution
(combined with high sensitivity) is the Key
capability for unique imaging studies in stellar and
extragalactic astrophysics.